281 research outputs found
Mock data study for next-generation ground-based detectors: The performance loss of matched filtering due to correlated confusion noise
The next-generation (3G/XG) ground-based gravitational-wave (GW) detectors such as Einstein Telescope (ET) and Cosmic Explorer (CE) will begin observing in the next decade. Due to the extremely high sensitivity of these detectors, the majority of stellar-mass compact-binary mergers in the entire Universe will be observed. It is also expected that 3G detectors will have significant sensitivity down to 2-7 Hz; the observed duration of binary neutron star signals could increase to several hours or days. The abundance and duration of signals will cause them to overlap in time, which may form a confusion noise that could affect the detection of individual GW sources when using naive matched filtering; matched filtering is only optimal for stationary Gaussian noise. We create mock data for CE and ET using the latest population models informed by the GWTC-3 catalog and investigate the performance loss of matched filtering due to overlapping signals. We find the performance loss mainly comes from a deviation in the noise's measured amplitude spectral density. The redshift reach of CE (ET) can be reduced by 15%-38% (8%-21%) depending on the merger rate estimate. The direct contribution of confusion noise to the total signal-to-noise ratio (SNR) is generally negligible compared to the contribution from instrumental noise. We also find that correlated confusion noise has a negligible effect on the quadrature summation rule of network SNR for ET, but might reduce the network SNR of high detector-frame mass signals for detector networks including CE if no mitigation is applied. For ET, the null stream can mitigate the astrophysical foreground. For CE, we demonstrate that a computationally efficient, straightforward single-detector signal subtraction method suppresses the total noise to almost the instrument noise level; this will allow for near-optimal searches
A mock data study for 3G ground-based detectors: the performance loss of matched filtering due to correlated confusion noise
The next-generation (3G/XG) ground-based gravitational-wave (GW) detectors
such as Einstein Telescope (ET) and Cosmic Explorer (CE) will begin observing
in the next decade. Due to the extremely high sensitivity of these detectors,
the majority of stellar-mass compact-binary mergers in the entire Universe will
be observed. It is also expected that 3G detectors will have significant
sensitivity down to 2-7 Hz; the observed duration of binary neutron star
signals could increase to several hours or days. The abundance and duration of
signals will cause them to overlap in time, which may form a confusion noise
that could affect the detection of individual GW sources when using naive
matched filtering; Matched filtering is only optimal for stationary Gaussian
noise. We create mock data for CE and ET using the latest population models
informed by the GWTC-3 catalog and investigate the performance loss of matched
filtering due to overlapping signals. We find the performance loss mainly comes
from a deviation in the noise's measured amplitude spectral density. The
redshift reach of CE (ET) can be reduced by 15-38 (8-21) % depending on the
merger rate estimate. The direct contribution of confusion noise to the total
SNR is generally negligible compared to the contribution from instrumental
noise. We also find that correlated confusion noise has a negligible effect on
the quadrature summation rule of network SNR for ET, but might reduce the
network SNR of high detector-frame mass signals for detector networks including
CE if no mitigation is applied. For ET, the null stream can mitigate the
astrophysical foreground. For CE, we demonstrate that a computationally
efficient, straightforward single-detector signal subtraction method suppresses
the total noise to almost the instrument noise level; this will allow for
near-optimal searches.Comment: 22 pages, 10 figures, comments are welcome, public code:
https://github.com/gwastro/confusion-noise-3
Aircraft Ground Taxiing Deduction and Conflict Early Warning Method Based on Control Command Information
Aircraft taxiing conflict is a threat to the safety of airport operations,
mainly due to the human error in control command infor-mation. In order to
solve the problem, The aircraft taxiing deduction and conflict early warning
method based on control order information is proposed. This method does not
need additional equipment and operating costs, and is completely based on
his-torical data and control command information. When the aircraft taxiing
command is given, the future route information will be deduced, and the
probability of conflict with other taxiing aircraft will be calculated to
achieve conflict detection and early warning of different levels. The method is
validated by the aircraft taxi data from real airports. The results show that
the method can effectively predict the aircraft taxiing process, and can
provide early warning of possible conflicts. Due to the advantages of low cost
and high accuracy, this method has the potential to be applied to airport
operation decision support system
Population Properties of Gravitational-Wave Neutron Star--Black Hole Mergers
Over the course of the third observing run of LIGO-Virgo-KAGRA Collaboration,
several gravitational-wave (GW) neutron star--black hole (NSBH) candidates have
been announced. By assuming these candidates are real signals and of
astrophysical origins, we analyze the population properties of the mass and
spin distributions for GW NSBH mergers. We find that the primary BH mass
distribution of NSBH systems, whose shape is consistent with that inferred from
the GW binary BH (BBH) primaries, can be well described as a power-law with an
index of plus a high-mass Gaussian component
peaking at . The NS mass spectrum could be shaped
as a near flat distribution between . The constrained NS
maximum mass agrees with that inferred from NSs in our Galaxy. If GW190814 and
GW200210 are NSBH mergers, the posterior results of the NS maximum mass would
be always larger than and significantly deviate from that
inferred in the Galactic NSs. The effective inspiral spin and effective
precession spin of GW NSBH mergers are measured to potentially have near-zero
distributions. The negligible spins for GW NSBH mergers imply that most events
in the universe should be plunging events, which supports the standard isolated
formation channel of NSBH binaries. More NSBH mergers to be discovered in the
fourth observing run would help to more precisely model the population
properties of cosmological NSBH mergers.Comment: 14 pages, 5 figures, 3 tables, accepted for publication in Ap
Improving the color yield of ink-jet printing on cationized cotton
This study examines the performance of digital ink-jet printing on cationized cotton treated with polyepichlorohydrin-dimethylamine (PECH-amine). The results show that the color yield of ink-jet printing with reactive inks on cationic modified cotton is much greater than that on untreated cotton. The effect on the increase of color yield by cationic modification is greater than that by preparation with alkali, urea, and thickener. The reason for this is that introducing positively charged sites increases dye uptake and dye fixation on cationized cotton. The results also show that cationic modification with PECH-amine decreases the rub fastness but increases the wash fastness of the treated cotton. <br /
Population Properties of Gravitational-wave Neutron Star-Black Hole Mergers
Over the course of the third observing run of the LIGO-Virgo-KAGRA Collaboration, several gravitational-wave (GW) neutron star-black hole (NSBH) candidates have been announced. By assuming that these candidates are real signals with astrophysical origins, we analyze the population properties of the mass and spin distributions for GW NSBH mergers. We find that the primary BH mass distribution of NSBH systems, whose shape is consistent with that inferred from the GW binary BH (BBH) primaries, can be well described as a power law with an index of α=4.8-2.8+4.5 plus a high-mass Gaussian component peaking at ∼33-9+14M⊙ . The NS mass spectrum could be shaped as a nearly flat distribution between ∼1.0 and 2.1 M ⊙. The constrained NS maximum mass agrees with that inferred from NSs in our Galaxy. If GW190814 and GW200210 are NSBH mergers, the posterior results of the NS maximum mass would be always larger than ∼2.5 M ⊙ and significantly deviate from that inferred in Galactic NSs. The effective inspiral spin and effective precession spin of GW NSBH mergers are measured to potentially have near-zero distributions. The negligible spins for GW NSBH mergers imply that most events in the universe should be plunging events, which support the standard isolated formation channel of NSBH binaries. More NSBH mergers to be discovered in the fourth observing run would help to more precisely model the population properties of cosmological NSBH mergers. © 2022. The Author(s). Published by the American Astronomical Society
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